skip to main content
OSTI.GOV title logo U.S. Department of Energy
Office of Scientific and Technical Information

Title: On Rapidly Rotating Magnetic Core-Collapse Supernovae

Abstract

The authors have analyzed magnetic effects which may occur in rapidly rotating core collapse supernovae. They consider effects from both magnetic turbulence and the formation of magnetic bubbles. For magnetic turbulence they have made a perturbative analysis for the spherically symmetric core-collapse supernova model that incorporates the build up of magnetic field energy in the matter accreting onto the proto-neutron star shortly after collapse and bounce. This significantly modifies the pressure profile and increases the heating of the material above the proto-neutron star resulting in an explosion even in rotating stars which would not explode otherwise. Regarding magnetic bubbles it is shown that a model with an initial uniform magnetic field ({approx} 10{sup 8}) gauss and uniform angular velocity of ({approx} 0.1 rad sec{sup -1}) can form magnetic bubbles due to the very non homologous nature of the collapse. It is estimated that the buoyancy of the bubbles causes matter in the proto-neutron star to rise, carrying neutrino-rich material to the neutron-star surface. This increases the neutrino luminosity sufficiently at early times to achieve a successful neutrino-driven explosion. Both magnetic mechanisms thus provide new means for initiating a Type II core-collapse supernova.

Authors:
; ;
Publication Date:
Research Org.:
Lawrence Livermore National Lab. (LLNL), Livermore, CA (United States)
Sponsoring Org.:
USDOE
OSTI Identifier:
15016858
Report Number(s):
UCRL-JRNL-208825
Journal ID: ISSN 0004-637X; ASJOAB; TRN: US0503755
DOE Contract Number:  
W-7405-ENG-48
Resource Type:
Journal Article
Journal Name:
Astrophysical Journal
Additional Journal Information:
Journal Volume: 628; Journal ID: ISSN 0004-637X
Country of Publication:
United States
Language:
English
Subject:
71 CLASSICAL AND QUANTUM MECHANICS, GENERAL PHYSICS; 72 PHYSICS OF ELEMENTARY PARTICLES AND FIELDS; 99 GENERAL AND MISCELLANEOUS//MATHEMATICS, COMPUTING, AND INFORMATION SCIENCE; ANGULAR VELOCITY; BUBBLES; EXPLOSIONS; HEATING; LUMINOSITY; MAGNETIC FIELDS; NEUTRINOS; STARS; SUPERNOVAE; TURBULENCE

Citation Formats

Wilson, J R, Mathews, G J, and Dalhed, H E. On Rapidly Rotating Magnetic Core-Collapse Supernovae. United States: N. p., 2004. Web.
Wilson, J R, Mathews, G J, & Dalhed, H E. On Rapidly Rotating Magnetic Core-Collapse Supernovae. United States.
Wilson, J R, Mathews, G J, and Dalhed, H E. 2004. "On Rapidly Rotating Magnetic Core-Collapse Supernovae". United States. https://www.osti.gov/servlets/purl/15016858.
@article{osti_15016858,
title = {On Rapidly Rotating Magnetic Core-Collapse Supernovae},
author = {Wilson, J R and Mathews, G J and Dalhed, H E},
abstractNote = {The authors have analyzed magnetic effects which may occur in rapidly rotating core collapse supernovae. They consider effects from both magnetic turbulence and the formation of magnetic bubbles. For magnetic turbulence they have made a perturbative analysis for the spherically symmetric core-collapse supernova model that incorporates the build up of magnetic field energy in the matter accreting onto the proto-neutron star shortly after collapse and bounce. This significantly modifies the pressure profile and increases the heating of the material above the proto-neutron star resulting in an explosion even in rotating stars which would not explode otherwise. Regarding magnetic bubbles it is shown that a model with an initial uniform magnetic field ({approx} 10{sup 8}) gauss and uniform angular velocity of ({approx} 0.1 rad sec{sup -1}) can form magnetic bubbles due to the very non homologous nature of the collapse. It is estimated that the buoyancy of the bubbles causes matter in the proto-neutron star to rise, carrying neutrino-rich material to the neutron-star surface. This increases the neutrino luminosity sufficiently at early times to achieve a successful neutrino-driven explosion. Both magnetic mechanisms thus provide new means for initiating a Type II core-collapse supernova.},
doi = {},
url = {https://www.osti.gov/biblio/15016858}, journal = {Astrophysical Journal},
issn = {0004-637X},
number = ,
volume = 628,
place = {United States},
year = {Mon Dec 20 00:00:00 EST 2004},
month = {Mon Dec 20 00:00:00 EST 2004}
}